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A KH instability rendered visible by clouds, known as fluctus, [2] over Mount Duval in Australia A KH instability on the planet Saturn, formed at the interaction of two bands of the planet's atmosphere Kelvin-Helmholtz billows 500m deep in the Atlantic Ocean Animation of the KH instability, using a second order 2D finite volume scheme
This is an image, captured in San Francisco, which shows the "ocean wave" like pattern associated with the Kelvin–Helmholtz instability forming in clouds. The Kelvin–Helmholtz instability (KHI) is an application of hydrodynamic stability that can be seen in nature. It occurs when there are two fluids flowing at different velocities.
The Kelvin–Helmholtz mechanism is an astronomical process that occurs when the surface of a star or a planet cools. The cooling causes the internal pressure to drop, and the star or planet shrinks as a result. This compression, in turn, heats the core of the star/planet.
This image is a derivative work of the following images: File:KHI.gif licensed with PD-self . 2009-09-20T03:20:33Z Bdubb12 479x240 (5608478 Bytes) {{Information |Description={{en|1=Numerical Simulation of Kelvin-Helmholtz instability found in nature, fluid dynamics, physics, etc. Turbulent mixing of two different density fluids is caused by a velocity difference or she
A Kelvin-Helmholtz instability forms where there's a velocity difference across the interface between two fluids: for example, wind blowing over water. You’ll often see the characteristic wave ...
In astrophysics, the thermal time scale or Kelvin–Helmholtz time scale is the approximate time it takes for a star to radiate away its total kinetic energy content at its current luminosity rate. [1]
As the instability grows, the center of mass of the fluid is lowered. In growing waves in the atmosphere, cold air moving downwards and equatorwards displaces the warmer air moving polewards and upwards. [citation needed] Baroclinic instability can be investigated in the laboratory using a rotating, fluid filled annulus. The annulus is heated ...
Hydrodynamics simulation of a single "finger" of the Rayleigh–Taylor instability. [1] Note the formation of Kelvin–Helmholtz instabilities, in the second and later snapshots shown (starting initially around the level =), as well as the formation of a "mushroom cap" at a later stage in the third and fourth frame in the sequence.